29.2 - Stars - s3.amazonaws.com
... form of light and heat • Appear to be tiny specks of white light • Most vary in color and are much larger than ...
... form of light and heat • Appear to be tiny specks of white light • Most vary in color and are much larger than ...
Lecture 17 Review
... The question is, what if the mass is greater than about 50 solar masses? If the forming star is too large, the gas cloud condenses quite fast, is unstable, gets very hot, and either explodes or fragments into smaller clouds which form individual stars. A second question is, can the mass of the gas ...
... The question is, what if the mass is greater than about 50 solar masses? If the forming star is too large, the gas cloud condenses quite fast, is unstable, gets very hot, and either explodes or fragments into smaller clouds which form individual stars. A second question is, can the mass of the gas ...
Word doc - UC-HiPACC - University of California, Santa Cruz
... Stars are born in groups or clusters when a cold giant molecular cloud collapses under its own gravitational force. If many stars form all at once—that is, if star formation efficiency is high—they will stay together as a gravitationally bound open cluster (like the Pleiades) or a globular cluster ( ...
... Stars are born in groups or clusters when a cold giant molecular cloud collapses under its own gravitational force. If many stars form all at once—that is, if star formation efficiency is high—they will stay together as a gravitationally bound open cluster (like the Pleiades) or a globular cluster ( ...
Life on the Main Sequence + Expansion to Red Giant
... composition) completely determines its properties. That’s why stars initially all line up along the main sequence. ...
... composition) completely determines its properties. That’s why stars initially all line up along the main sequence. ...
General Introduction 1. Luminosity, Flux and Magnitude The
... The evolution of the Sun is shown schematically in Fig. 7.3. The red giant phase occurs after the interior of the Sun is exhausted of hydrogen and helium burning initiates. The Sun is not massive enough to burn elements beyond He, so after shedding roughly half its mass in a violent wind leading to ...
... The evolution of the Sun is shown schematically in Fig. 7.3. The red giant phase occurs after the interior of the Sun is exhausted of hydrogen and helium burning initiates. The Sun is not massive enough to burn elements beyond He, so after shedding roughly half its mass in a violent wind leading to ...
Astronomy PPT
... “warm” colors and blue may be thought of as a “cool” color, scientists consider the opposite. ...
... “warm” colors and blue may be thought of as a “cool” color, scientists consider the opposite. ...
Lecture10
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
... not too hot and not too cold, many hydrogen atoms have their electron in the n = 2 orbit: hence strong absorption ...
Lecture 13
... The UBVRI system • In the 1960s, Johnson (and later others) extended the UBV system to the red and infrared, with R,I,J,K,L,M,N.... bands. • In the optical, then, we have the UBVRI broadband system. • It was found that the UBV system did not work well for very cool stars, like K and M spectral type ...
... The UBVRI system • In the 1960s, Johnson (and later others) extended the UBV system to the red and infrared, with R,I,J,K,L,M,N.... bands. • In the optical, then, we have the UBVRI broadband system. • It was found that the UBV system did not work well for very cool stars, like K and M spectral type ...
3 - MrFuglestad
... Red Giant – Hydrogen fusion ends in the core, but continues in a layer just outside the Helium core. The outer layers of the star expand because the area of Hydrogen being fused pushes the outer layers out. These outer layers cool and become less luminous. Therefore there is a change in size and co ...
... Red Giant – Hydrogen fusion ends in the core, but continues in a layer just outside the Helium core. The outer layers of the star expand because the area of Hydrogen being fused pushes the outer layers out. These outer layers cool and become less luminous. Therefore there is a change in size and co ...
Chapter 8 powerpoint presentation
... is we obtain a spectrum for a star of unknown distance. We use the spectrum to determine the spectral type, which locates it on the x-axis of the H-R diagram. Now draw a line up to the main sequence, and continue it horizontally to determine it’s absolute magnitude, Mv. The absolute magnitude combin ...
... is we obtain a spectrum for a star of unknown distance. We use the spectrum to determine the spectral type, which locates it on the x-axis of the H-R diagram. Now draw a line up to the main sequence, and continue it horizontally to determine it’s absolute magnitude, Mv. The absolute magnitude combin ...
HR Diagram
... H-R Diagram Scientists began to learn about stars by observing properties of stars, including brightness and color. Astronomers tried to make sense of the star data by grouping together stars with similar properties. The Hertzsprung-Russell diagram provides a way to group similar stars. The H-R dia ...
... H-R Diagram Scientists began to learn about stars by observing properties of stars, including brightness and color. Astronomers tried to make sense of the star data by grouping together stars with similar properties. The Hertzsprung-Russell diagram provides a way to group similar stars. The H-R dia ...
Picture: Alnitak is the left-hand star in Orion`s Belt. Image: NASA
... 3500 - 5000 K Yellow - orange stars ...
... 3500 - 5000 K Yellow - orange stars ...
Integrative Studies 410 Our Place in the Universe
... The stars, Sun, Moon and planets rotate us There is no apparent curvature of the ground The Milky Way is a band that surrounds us There are no signs for any movement of the ...
... The stars, Sun, Moon and planets rotate us There is no apparent curvature of the ground The Milky Way is a band that surrounds us There are no signs for any movement of the ...
Review Questions for Exam #2
... In order to figure out the mass of a star we observe binary star systems and use Kepler’s 3rd Law, (M1 + M2) P2 = 4π2*a3/G Discuss how we determine, P and a. How do we solve for individual mass (like M1) rather than (M1 + M2)? ...
... In order to figure out the mass of a star we observe binary star systems and use Kepler’s 3rd Law, (M1 + M2) P2 = 4π2*a3/G Discuss how we determine, P and a. How do we solve for individual mass (like M1) rather than (M1 + M2)? ...
Lecture 13
... No White Dwarf Can have more than 1.4M Otherwise it will groan and collapse under its own weight. We’ll come back to this later. ...
... No White Dwarf Can have more than 1.4M Otherwise it will groan and collapse under its own weight. We’ll come back to this later. ...
Energy Transport
... star to contract causing temp to increase again because of energy release from gravity. • If energy production were to be too much then the steps would occur in reverse. ...
... star to contract causing temp to increase again because of energy release from gravity. • If energy production were to be too much then the steps would occur in reverse. ...
Section 25.2 Stellar Evolution
... Stars less than one-half the mass of the sun never evolve to the red giant stage but remain in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. Death of Medium-Mass Stars Stars with masses similar to the sun evolve in essentially the same ...
... Stars less than one-half the mass of the sun never evolve to the red giant stage but remain in the stable main-sequence stage until they consume all their hydrogen fuel and collapse into a white dwarf. Death of Medium-Mass Stars Stars with masses similar to the sun evolve in essentially the same ...
Powerpoint Presentation (large file)
... 2. Why are red giants larger than main-sequence stars? 3. Do all stars evolve into red giants at the same rate? 4. How do we know that many stars lived and died before our Sun was born? 5. Why do some giant stars pulsate in and out? 6. Why do stars in some binary systems evolve in unusual ways? ...
... 2. Why are red giants larger than main-sequence stars? 3. Do all stars evolve into red giants at the same rate? 4. How do we know that many stars lived and died before our Sun was born? 5. Why do some giant stars pulsate in and out? 6. Why do stars in some binary systems evolve in unusual ways? ...
What is an atom?
... In the last chapter you read how telescopes gather starlight and how spectrographs spread out the light into spectra. Now you are ready to see what all the fuss is about. Here you will find answers to four ...
... In the last chapter you read how telescopes gather starlight and how spectrographs spread out the light into spectra. Now you are ready to see what all the fuss is about. Here you will find answers to four ...
Review for Exam 2
... 2) What do all stars on the main sequence have in common? How does the 6me spent on the main sequence depend on mass? 3) What are the evolu6onary stages of stars of high-‐ and low-‐mass stars ...
... 2) What do all stars on the main sequence have in common? How does the 6me spent on the main sequence depend on mass? 3) What are the evolu6onary stages of stars of high-‐ and low-‐mass stars ...
Document
... On the back of your graphic organizer/note handout, there is an essential question regarding the energy of a star and the lifetime of the star. Create a hypothesis to the question, then look at the data provided to pull out specific evidence, write a justification of why you pulled that ...
... On the back of your graphic organizer/note handout, there is an essential question regarding the energy of a star and the lifetime of the star. Create a hypothesis to the question, then look at the data provided to pull out specific evidence, write a justification of why you pulled that ...
Stellar Birth - Chabot College
... How do stars form? How do we know? How will our Sun evolve as a star? What will its final state be? Compare its predicted evolution to that of higher-mass stars. How do they end? How do we know? ...
... How do stars form? How do we know? How will our Sun evolve as a star? What will its final state be? Compare its predicted evolution to that of higher-mass stars. How do they end? How do we know? ...
File
... the atoms to move closer. This starts a process called fusion. Fusion occurs when the atoms are so close together that they start to combine, making helium from hydrogen. When this happens, energy is created and a new star is formed! ...
... the atoms to move closer. This starts a process called fusion. Fusion occurs when the atoms are so close together that they start to combine, making helium from hydrogen. When this happens, energy is created and a new star is formed! ...
Astronomy 242: Review Questions #1 Distributed: February 10
... (a) Using the information in this diagram, estimate the range of surface gravities g for stars along the Main Sequence. Which end of the main sequence has the highest surface gravities? (b) Typical white dwarf stars have masses Mwd ≃ 1M⊙ . How do the surface gravities of white dwarf stars compare to ...
... (a) Using the information in this diagram, estimate the range of surface gravities g for stars along the Main Sequence. Which end of the main sequence has the highest surface gravities? (b) Typical white dwarf stars have masses Mwd ≃ 1M⊙ . How do the surface gravities of white dwarf stars compare to ...
Stellar classification
In astronomy, stellar classification is the classification of stars based on their spectral characteristics. Light from the star is analyzed by splitting it with a prism or diffraction grating into a spectrum exhibiting the rainbow of colors interspersed with absorption lines. Each line indicates an ion of a certain chemical element, with the line strength indicating the abundance of that ion. The relative abundance of the different ions varies with the temperature of the photosphere. The spectral class of a star is a short code summarizing the ionization state, giving an objective measure of the photosphere's temperature and density.Most stars are currently classified under the Morgan–Keenan (MK) system using the letters O, B, A, F, G, K, and M, a sequence from the hottest (O type) to the coolest (M type). Each letter class is then subdivided using a numeric digit with 0 being hottest and 9 being coolest (e.g. A8, A9, F0, F1 form a sequence from hotter to cooler). The sequence has been expanded with classes for other stars and star-like objects that do not fit in the classical system, such class D for white dwarfs and class C for carbon stars.In the MK system a luminosity class is added to the spectral class using Roman numerals. This is based on the width of certain absorption lines in the star's spectrum which vary with the density of the atmosphere and so distinguish giant stars from dwarfs. Luminosity class 0 or Ia+ stars for hypergiants, class I stars for supergiants, class II for bright giants, class III for regular giants, class IV for sub-giants, class V for main-sequence stars, class sd for sub-dwarfs, and class D for white dwarfs. The full spectral class for the Sun is then G2V, indicating a main-sequence star with a temperature around 5,800K.